Understandably, the cluster mass is a key parameter for studies that aim to constrain cosmological parameters using galaxy cluster distribution with mass and redshift, i.e. galaxy cluster number density. The cluster mass, however, is not directly observable and there are several ways to infer it via observations under simple theoretical assumptions. Each of these ways to infer the mass is prone to a bias and intrinsic scatter associated with the observations being used. The cluster mass can be estimated using the hydrostatic equilibrium (HE) equation under the assumption of the cluster having a spherical Dark Matter halo; the Intra Cluster Medium (ICM) profiles, namely, the density profile from X–ray and the pressure profile from the Sunyaev–Zeldovich (SZ) effect [1]} observations, can be combined to infer the cluster mass (see e.g. [2]}). This inference is prone to mass bias associated to the assumptions made for the HE equation. The kinematic studies of the member galaxies can also be used to estimate the mass of galaxy clusters (see e.g. [3]}). These calculations require spectral information of a lot of member galaxies to get an accurate mass estimate with good precision. Estimating the cluster mass through measuring the gravitational lensing effect of clusters on the background sources is one of the least biased methods but, comes with high dispersion on the mass estimate [4]}. Finally, another way to infer the cluster mass is through scaling laws, which, when correctly calibrated, relate the mass to observational quantities, such as X–ray luminosity, SZ brightness, etc. [5]}, [6]}, [7]}, [8]}, [9]}. An alternative and orthogonal approach to refine the cluster mass estimates is by using state–of–the–art N–body hydrodynamical simulations as useful and efficient test–beds to increase our theoretical understanding [10]}. Evidently, it is critical to understand astrophysical details that may affect the mass estimation via the observational methods mentioned above and to properly calibrate scaling relations between observables and the mass of the cluster.
